Current understandings on dust formation in supernovae

Takaya Nozawa(NAOJ, Division of theoretical astronomy)

2014/06/25

Main collaborators: Masaomi Tanaka (NAOJ, theory)

Keiichi Maeda (Kyoto University)

Takashi Kozasa, Asao Habe (Hokkaido University)

Hideyuki Umeda (University of Tokyo)

Ken’ichi Nomoto (Kavli IPMU)

‐ Formation of dust in the ejecta of supernovae

‐ Dynamics, destruction, and heating of dust grains

in high-velocity shock waves

‐ Evolution of grain size distribution in galaxies and

interstellar extinction curves

‐ Origin of dust grains in the early universe and the

roles of dust in star formation

‐ Formation of dust in stellar winds and mass-loss

history at late phases of stellar evolution

0-1. My research interests

0-2. Introduction ・ SNe are important sources of interstellar

dust?

・ abundant metal (metal : N > 5) ・ low temperature (T < ~2000 K) ・ high density (n > ~106 cm-3)

‐huge amounts of dust grains (>108 Msun) are detected in host galaxies of quasars at redshift z > 5 ➔ 0.1 Msun of dust per SN is needed to explain such massive dust at high-z (e.g. Dwek et al. 2007)

‐contribution of dust mass from AGB stars and SNe

n(AGB stars) / n(SNe) ~ 10-20 Mdust = 0.01-0.05 Msun per AGB (Zhukovska & Gail 2008)

Mdust = 0.1-1.0 Msun per SN (e.g., Nozawa et al. 2003, 2007)

mass-loss windsof AGB starsexpanding ejectaof supernovae

at ~1 days

H-envelopeHe-core

NS or BH

He–layer (C>O)O–Ne-Mg layerSi–S layer

Fe–Ni layer

Dust formation at ~1-3 years

after explosion

Dust Formation in the ejecta of SNe

1. Observations of Dust Formation

in SNe (and SNRs)

1-1. Summary of observed dust mass in CCSNe

missing cold dust?

Far-IR to sub-mm observations are essential for revealing the mass of dust grains produced in the ejecta of SNe

supernovae

young SNRs

swept-up IS dust?

Matsuura+2011Balow+2010 Gomez+2012

1-2. Herschel detects cool dust in SN 1987A

Herschel detects cool (~20K) dust of ~0.4-0.7 Msun toward SN 1987A!

on 4 Oct 2003Gemini T-ReCS(λ = 10.36 μm)2 pixels : 0.18”(Bouchet+04)

Matsuura+2011

~180K~10-5 Msun

~20K~0.5 Msun

1-3. Resolving cool dust in SN 87A with ALMA Band 9 (450 μm)Band 7 (850 μm)

0.1 Msun of silicate ➔ 5σ detection at Band 9 !!

2 arcsec

ALMA Cycle 0 Proposal‘Detecting cool dust in SN1987A’ （ TN, Tanaka, et al.)

CASA simulationwith extended config. (4 hrs)

This proposal was ranked in the highest priority !!

1-4. Successful ALMA proposals for SN 1987A

Band 9extended configuration

Band 3, 6, 7, 9compact configuration

Our proposal was not executed

1-5. ALMA reveals dust formed in SN 1987A

ALMA spatially resolves cool (~20K) dust of ~0.5 Msun formed in the ejecta of SN 1987A ➔ SNe could be production factories of dust grains

SED of 25-years old SN 1987A

Indebetouw+2014

blue: Hα green: 1.6 µm red: CO(2-1)

➜ >0.1 Msun of CO

Barlow+10, A&A, 518, L138

1-6. Possible target: SNR 1E0102-72.3 in SMC

Stanimirovic+05

100 μm ・ Cassiopeia A - O-rich (Type IIb) - age : 330 yr - Mwarm < 10-2 Msun

- Mcool ~ 0.07 Msun

Cas A model (Nozawa+10)

・ SNR 1E0102-72.3 - O-rich (Type Ib?) - age : ~1000 yr - Mwarm ~ 10-3 Msun

- Mcool ~ ???

24 μm

Gaetz+00

24 μm X-ray, radio

young (compact) supernova remnants in LMC/SMC !

40 arcsec

Band 9 with ACA

Band 3 with ACA

Band 3

1-7. SNR 1E0102-72.3 is too extended!

SN 1987A

1-8. Flux estimates necessary for detection

1987ABand 9

1E0102Band 9 full operation

1 sigma, 1 hr

effective flux(flux per beam)

1-9. Summary of observations of SN dust

‐ALMA confirmed the presence of huge amounts of newly formed dust in the ejecta of SN 1987A ➜ heavy elements (Si, Mg, Fe, C) are locked up in dust grains ➜ SNe are main production factories of dust grains

‐ It seems too hard to detect thermal emission from cool dust in any other SNe/SNRs with ALMA ➜ young SNRs in LMC/SMC are too extended

‐A part of dust grains formed in the SN ejecta will be destroyed by the reverse shocks

what fraction of dust grains can survive to be injected? ➜ destruction efficiency depends on dust composition and size ➜ infrared to submm observations have few information on the the composition and size distribution of dust

FSHe core

RSCD

T = (1-2)x104 KnH,0 = 0.1-1 cm-3

Evolution of dust in SN remnants

2. Theoretical Studies on Dust

Formation in SNe

2-1. Dust formation in primordial SNeNozawa+2003, ApJ, 598, 785

‐nucleation and grain growth theory (Kozasa & Hasegawa 1987)

‐no mixing of elements within the He-core

‐complete formation of CO and SiO

〇 Population III SNe model (Umeda & Nomoto 2002)

　 ‐ SNe II ： MZAMS = 13, 20, 25, 30 Msun (E51=1)

‐ PISNe ： MZAMS = 170 Msun (E51=20), 200 Msun (E51=28)

2-2. Dust formed in Type II-P SNe

‐a variety of grain species can 　 condense according to elemental composition in each layer

‐ condensation time: 300-600d after explosion

‐ average grain radii: >~0.01 μm

average radius

0.01 μm

condensation time

Nozawa+03, ApJ, 598, 785

C / O < 1 ➔ all C atoms are locked up in CO

C / O > 1 ➔ all O atoms are locked up in CO

2-3. Size distribution of newly formed dustNozawa+2003, ApJ, 598, 785

‐C, SiO2, and Fe grains have lognormal-like size distribution, while the other grains have power-law size distribution

‐The composition and size distribution of dust formed are almost independent of types of supernova ## average grain radius is smaller for PISNe than SNe II-P

‐Total mass of dust is higher for a higher progenitor mass (MZAMS) SNe II ： mdust = 0.1-1.5 Msun, mdust / mmetal = 0.2-0.3 PISNe ： mdust = 10-30 Msun, mdust / mmetal = 0.3-0.4

‐almost all Fe, Mg, and Si are locked up in dust grains, while most of C and O remain in the gas-phase (such as CO) ➔ dust-to-metal mass ratio is not high for SNe II

SNe II

2-4. Total mass of dust formed in the ejecta

2-5. Temperature and density of gas in SNRs

Model : Mpr= 20 Msun (E51=1)

nH,0 = 1 cm-3

The temperature of the gas swept up by the shocks ➔ 106-108 K ↓ Dust grains residing in the shocked hot gas are eroded by sputtering

Downward-pointing arrows: forward shock in upper panel reverse shock in lower panel

Nozawa+07, ApJ, 666, 955

2-6. Evolution of dust in SNRs

Dust grains in the He core collide with reverse shock at (3-13)x103 yr

The evolution of dust heavilydepends on the initial radius and composition

aini = 0.01 μm (dotted lines) ➔ completely destroyed

aini = 0.1 μm (solid lines) ➔ trapped in the shell

aini = 1 μm (dashed lines) ➔ injected into the ISM

Model : Mpr= 20 Msun (E51=1)

nH,0 = 1 cm-3

Nozawa+07, ApJ, 666, 955

2-7. Dust mass and size ejected from SN II-P

total mass of dust surviving the destruction in Type II SNRs; 0.07-0.8 Msun (nH,0 = 0.1-1 cm-3)

size distribution of dust after theshock-destruction is domimated by large grains (> 0.01 μm)

SNe II at time of dust formation

after destruction of dustby reverse shock

PISNe Nozawa+07, ApJ, 666, 955

‐Various grain species can condense in the ejecta

➔ almost all Fe, Mg, and Si are locked up in grains

‐The fate of newly formed dust within SNRs strongly

depends on the initial radii and compositions

‐The size distribution of dust surviving the destruction in SNRs is weighted to relatively large size (> 0.01 μm).

‐The total mass of dust injected into the ISM decreases with increasing the ambient gas density

for nH,0 = 0.1-1 cm-3

SNe II-P ➔ Mdust = 0.1-0.8 Msun

➔ making significant contribution to dust budget

2-8. Summary of dust production in SNe